adsabs/AstroCLIMB huggingface dataset:
Paper: Discovery of a Radio-loud Narrow-line Seyfert 1 Galaxy at z = 0.9 Reddened with a Strong 2175 Å Bump
Authors: Yipeng Zhou, Lei Hao, Peng Jiang, Xiang Pan, Luming Sun, Chichuan Jin, Xuejie Dai, Wenjuan Liu, Tuo Ji, Zhenya Zheng, Xiangning Huang, Xiheng Shi, Yibo Wang, Yifei Xiong, Chenwei Yang
Figure caption: Dereddened spectrum of J1605+4743 (black) using the model extinction curve shown in Figure 2, in comparison with the scaled spectrum of J1105+0457 (green). The dashed blue curve is the featureless continuum fitted by a power law with a spectral index of α = −2 (f  λ  ∝ λ  α ). The orange curve shows the best-fit model of Fe II emission lines by the template extracted from the prototype narrow-line-Seyfert 1 galaxy, IZw 1. Identified emission/absorption lines are labeled above/below the data (tentative identifications are marked with “?”). Note the close resemblance between the spectra of J1605+4743 and J1105+0457.
Paper: Discovery of a Radio-loud Narrow-line Seyfert 1 Galaxy at z = 0.9 Reddened with a Strong 2175 Å Bump
Authors: Yipeng Zhou, Lei Hao, Peng Jiang, Xiang Pan, Luming Sun, Chichuan Jin, Xuejie Dai, Wenjuan Liu, Tuo Ji, Zhenya Zheng, Xiangning Huang, Xiheng Shi, Yibo Wang, Yifei Xiong, Chenwei Yang
Figure caption: Left: best-fit COG using the seven Fe II absorption lines (red dots) is shown in the thick black line, and its 1σ deviations are shown as gray lines. Column densities of other ions are estimated using the best-fit COG based on the measured equivalent widths (blue dots). See Section 4 for a detailed description. Right: the best-fit Fe II column density and Doppler parameter for the COG (filled red circle). The 1, 2, and 3σ confidence levels are shown in black contours.
Paper: Discovery of a Radio-loud Narrow-line Seyfert 1 Galaxy at z = 0.9 Reddened with a Strong 2175 Å Bump
Authors: Yipeng Zhou, Lei Hao, Peng Jiang, Xiang Pan, Luming Sun, Chichuan Jin, Xuejie Dai, Wenjuan Liu, Tuo Ji, Zhenya Zheng, Xiangning Huang, Xiheng Shi, Yibo Wang, Yifei Xiong, Chenwei Yang
Figure caption: The observed absorption lines (black stepped lines) and their best-fit Gaussian models in their common velocity spaces in the quasar rest frame.
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Relation between the dynamical mass of the host galaxies and the mass of the central black holes of the z ≳ 5.7 quasars for the X–shooter/ALMA sample (orange diamonds, with right pointing orange triangles indicating lower limits; see also Neeleman et al. 2021) and for other studies (violet circles). The typical error (including systematics) is shown as a cross in the top-left corner. For comparison, the best fit of the relation between M BH and M Bulge derived by Kormendy & Ho (2013) is shown as a gray dashed line. The extrapolation of the M BH/M Host ratio evolution derived by Decarli et al. (2010b) for z ∼ 6.3 (the median redshift of the quasar sample) is shown as an orange dashed line. Light-gray points are data for 66 local galaxies derived by Savorgnan et al. (2016). The bottom panel highlights the differences with respect to the local relation by re-scaling the y-axis by a factor of 100. Histograms in the right panel show the black hole mass distributions for local galaxies (in gray) and for high-redshift quasars (in orange and pink).
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Evolutionary tracks of black hole seeds (purple lines) to reach the observed quasar masses at z ∼ 6 (orange diamonds and pink circles). These are calculated using Equation (5) with parameters: f duty = 1, ϵ = 0.1, λ Edd = 1, and t Sal = 45 Myr. Mass ranges for different black hole seed formation scenarios are indicated by shaded regions. For the sake of comparison, gray contours and points indicate the location of 1.3 < z < 2.3 SDSS DR7 quasars (Shen et al. 2011). In the right panel, we show the cumulative distributions of observed black holes (orange and pink for the z ∼ 6 quasars, and black for the 0.34 < z < 2.30 quasars) and expectations for the considered evolutionary pathway starting at z = 30 (purple).
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Distribution of z ≳ 5.7 quasars in the circular velocity vs. black hole mass plane. Circular velocities are derived from the 1D velocity dispersion of the Lyα halos considering ﹩{V}_{{\rm{c}}}=\sqrt{2}{\sigma }_{\mathrm{Ly}\alpha }^{\mathrm{Halo}}﹩. Black hole masses and circular velocities for local galaxies are taken from the review of Kormendy & Ho (2013; gray points). The gray dashed line is the best fit to the z ∼ 0 data following the procedure in Volonteri et al. (2011). Histograms in the right panel show the distribution of black hole masses of the high-redshift and local samples. The color code is the same as in Figure 11.
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Black hole masses (bottom) and Eddington ratios (top) of quasars from the X–shooter /ALMA sample (20 targets) and from the literature (five targets) as a function of total Ly α luminosity of the extended halo. The color code of the points is the same as in Figure 5, and left pointing triangles indicate upper limits on the Lyα halo luminosities. Median values calculated after splitting the sample at a halo luminosity of 1043 erg s−1 are shown as blue pentagons. The 16th and 84th percentiles of the distribution are shown as error bars along the y-axis. Error bars along the x-axis indicate the luminosity range covered by each bin. Histograms in the right panel show the distribution of black hole masses and Eddington ratios considered.
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Logarithmic Eddington ratio distributions of the quasars observed at <0.″25 resolution with ALMA by Neeleman et al. (2021). Host galaxies that show disturbed and undisturbed [C II] 158  μm morphologies are shown in the upper and lower panels, respectively. For the sake of comparison, the Eddington ratios of the luminosity-matched samples are also shown in black. However, note that no information on the hosts is taken into account for the selection of the z ∼ 0.3 − 2.3 quasars. The box plots at the top of each panel mark the median values of the various distributions. High-redshift quasars residing in galaxies with a disturbed morphology have a median Eddington ratio higher than those in undisturbed hosts. However, the two distribution do not differ enough to suggest differences between their parent populations. The color code is the same as in Figure 6.
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Redshift distribution of (from top to bottom) bolometric luminosities, black hole masses, and Eddington ratios for bright (M1450 < −25.2 mag) z ≳ 5.7 quasars (color coded as in Figure 5). Blue pentagons mark median values in three redshift bins. Error bars on the y-axis represent the 16th and the 84th percentiles of the distribution, while on the x-axis they indicate the size of the redshift bin. For comparison, the distribution of the luminosity-matched sample is also shown by gray contours.
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Same as Figure 9 but for different black hole growth parameters.
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Comparison of FWHM measurements of the Mg II (orange diamonds) and C IV (purple triangles) lines (left panel) and black hole mass estimates (right panel) for the five quasars in common between our X–shooter sample and that of Shen et al. (2019). The relative differences between two measurements are showed in the bottom panels.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: Magnetic field energy per unit mass ﹩{{ \mathcal E }}_{B}={v}_{{\rm{A}}}^{2}/2﹩ (solid line) and turbulent kinetic energy per unit mass ﹩{{ \mathcal E }}_{\mathrm{tur}.}={v}_{\mathrm{tur}}^{2}/2﹩ (dashed line) as a function of time. The calculation uses the maximum magnetic field strength and its corresponding density and turbulent velocity. The energies are normalized by the initial magnetic field energy ﹩{{ \mathcal E }}_{{B}_{0}}﹩. The dashed–dotted line denotes the analytical prediction derived in Xu & Lazarian (2016).
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: The ratios of the maximum values of density, (total) velocity, magnetic field, and pressure to their initial values in the postshock region as a function of time.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: The distributions of averaged (along the z-axis) postshock magnetic field strength, 〈M s〉, and 〈M A〉 in the vicinity of the shock front. M s is the ratio of total velocity to sound speed, while M A is the ratio of turbulent velocity to Alfvén speed. The snapshot reaches t ≈ 0.75t shock. Short white lines indicate the magnetic field orientations.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: The ratio of the averaged magnetic field to its initial value over the postshock’s turbulent shell as a function of time.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: Averaged (over the y-axis and z-axis) profiles of 〈M A〉 as a function of x using the snapshot at t ≈ 0.75t shock.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: Comparison of the energy spectrum of the postshock turbulent magnetic field obtained from 3D simulation (1024 × 512 × 512 cells; bottom) and 2D simulation (1024 × 512 × 1 cells; top) at t ≈ 0.75t shock. Note that we consider the spectrum only on the k  x  = 0 plane in Fourier space. Therefore, we have the slope ≈−4 + (D − 1) and ≈−11/3 + (D − 1) for compressive and solenoidal turbulence, respectively. Here D = 2 stands for 3D simulation and D = 1 is for 2D simulation.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: The histogram of the amplified magnetic field strength in the postshock’s turbulent shell.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: The maps of gas density, total velocity, magnetic field, and pressure. The 2D simulation cube β = 10 at t ≈ 0.75t shock is used here. Mean magnetic field is parallel to the x-axis. The physical variables are expressed in terms of numerical units.
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Temperature dependence of the rate coefficient ﹩{k}_{{{\rm{N}}}^{+}}^{{{\rm{D}}}_{2}}﹩ of the reaction of N+ ions with D2. Upper panel: raw data and correction. The temperature dependence of the reaction rate coefficients ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{g}}\text{-}{{\rm{D}}}_{2}}﹩ and the binned and averaged data are indicated by small points and stars, respectively. The full and open squares indicate ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HD}}﹩ and ﹩{f}_{{\rm{g}}\text{-}{{\rm{D}}}_{2}}^{{\rm{H}}{\rm{D}}}{k}_{{{\rm{N}}}^{+}}^{{\rm{H}}{\rm{D}}}﹩, respectively. The full circles indicate the temperature dependence of ﹩{k}_{{{\rm{N}}}^{+}}^{{{\rm{D}}}_{2}}﹩ obtained after the correction of ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{g}}\text{-}{{\rm{D}}}_{2}}﹩ for the admixture of HD in D2 gas by subtracting ﹩{f}_{{\rm{g}}\text{-}{{\rm{D}}}_{2}}^{{\rm{H}}{\rm{D}}}{k}_{{{\rm{N}}}^{+}}^{{\rm{H}}{\rm{D}}}﹩. The error bars of ﹩{k}_{{{\rm{N}}}^{+}}^{{{\rm{D}}}_{2}}﹩ account also for the 20% systematic error of ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HD}}﹩. Lower panel: comparison of the present data with the temperature dependence of ﹩{k}_{{{\rm{N}}}^{+}}^{{{\rm{D}}}_{2}}﹩ obtained by Gerlich (1993; 22PT), Tosi et al. (1994; MB and CB), Marquette et al. (1988; CRESU), Ervin & Armentrout (1987; GIB), and Adams & Smith (1985; SIFDT). In both panels, the full line indicates the fit of the temperature dependence of ﹩{k}_{{{\rm{N}}}^{+}}^{{{\rm{D}}}_{2}}﹩ by the Arrhenius function with a constant background term (see text).
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Temperature dependencies of the reaction rate coefficients ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDa}}﹩ for the production of ND+ (circles) and ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDb}}﹩ for the production of NH+ (full diamonds). The uncorrected values ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{g}}\text{-}{\rm{H}}{\rm{D}}{\rm{b}}}﹩ (open diamonds) are shown for comparison. The dashed curve and the filled area indicate the temperature dependence and uncertainty in the product ﹩{f}_{{\rm{g}}\text{-}{\rm{H}}{\rm{D}}}^{{{\rm{H}}}_{2}}{k}_{{{\rm{N}}}^{+}}^{{\rm{n}}\text{-}{{\rm{H}}}_{2}}﹩, which was used to correct ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{g}}\text{-}{\rm{H}}{\rm{D}}{\rm{b}}}﹩ for the admixture of H2 in the HD gas (﹩{f}_{{\rm{g}}\text{-}{\rm{H}}{\rm{D}}}^{{{\rm{H}}}_{2}}=0.015\pm 0.015﹩). We also indicate the values of ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDa}}﹩ and ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDb}}﹩ measured by Adams & Smith (1985; SIFDT) and Ervin & Armentrout (1987; GIB); the overall reaction rate coefficient ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HD}}﹩ measured by Gerlich (1992b; 22PT); and ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDa}}﹩ measured by Marquette et al. (1988; CRESU) and calculated by Grozdanov et al. (2016; PST).
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Upper panel: measured temperature dependence of the rate coefficient ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{g}}\text{-}{\rm{H}}{\rm{D}}}﹩ of the reaction of N+ with the HD gas. The raw data without binning are indicated with the small points. The stars indicate the binned values. Lower panel: measured temperature dependence of the product branching ratio ﹩{{\rm{B}}{\rm{R}}}_{{{\rm{N}}{\rm{H}}}^{+}}^{{\rm{g}}\text{-}{\rm{H}}{\rm{D}}}﹩ for the production of NH+. The raw data are indicated with the smaller points, and the stars indicate the binned values. The diamonds indicate the values of ﹩{\mathrm{BR}}_{{\mathrm{NH}}^{+}}^{\mathrm{HD}}﹩ obtained after the correction for the presence of up to 3% of normal H2 in the used HD gas.
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Arrhenius plot of the temperature dependence of the reaction rate coefficient ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDa}}﹩. The fit of the temperature dependence of ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDa}}﹩ (for T < 55K) by the Arrhenius function, ﹩k(T)=A\exp (-{E}_{{\rm{A}}}/{k}_{{\rm{B}}}T)﹩, is indicated by a full straight line (with extrapolation to higher temperatures indicated by the dotted line). The fit of all present data by the modified Arrhenius function ﹩k{(T)=A(T/300\,{\rm{K}})}^{\beta }\exp (-{E}_{{\rm{A}}}/{k}_{{\rm{B}}}T)﹩ is indicated by the dashed line. The dashed–dotted line indicates the Arrhenius fit by Marquette et al. (1988) used in astrochemical models. The values of ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDa}}﹩ previously calculated by Grozdanov et al. (2016; PST) and measured by Marquette et al. (1988; CRESU), Adams & Smith (1985; SIFDT), and Ervin & Armentrout (1987; GIB) are also indicated.
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Measured time evolutions of the normalized numbers (﹩{n}_{x}(t)/{n}_{{{\rm{\Sigma }}}_{0}}﹩) of the primary N+ ions and of the produced ND+ and NH+ ions. The solid lines are fits of the measured data. The measurements were performed at the collisional temperature T = 126 K. The helium number density is [He] = 1.6 × 1013 cm−3. Upper panel: time evolutions measured for a low density of the reactant gas, [g-HD] = 5.0 × 1010 cm−3. The amount of secondary ﹩{\mathrm{NH}}_{2}^{+}﹩ ions estimated from the fit is indicated by the dotted line. The branching ratio determined from the fit is ﹩{\mathrm{BR}}_{{{NH}}^{+}}=0.04﹩. Lower panel: time evolutions measured for a high density of the reactant gas, [g - HD] = 5.4 × 1011 cm−3. The fitted reaction rate coefficient is ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{g}}\text{-}{\rm{H}}{\rm{D}}}=4.2\,\times {10}^{-10}\,{{\rm{c}}{\rm{m}}}^{3}\,{{\rm{s}}}^{-1}﹩.
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Arrhenius plot of the temperature dependence of the reaction rate coefficients ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDb}}﹩ (closed diamonds) obtained after correction for the presence of normal H2 in the HD gas (﹩{f}_{{\rm{g}}\text{-}{\rm{H}}{\rm{D}}}^{{{\rm{H}}}_{2}}=0.015\pm 0.015﹩). The fit of the obtained temperature dependence of ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDb}}﹩ by the Arrhenius function ﹩k(T)\,=A\exp (-{E}_{{\rm{A}}}/{k}_{{\rm{B}}}T)+{k}_{\mathrm{bg}})﹩ is indicated by the solid line. The temperature range of the fit is 50—250 K. Indicated are values of ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDb}}﹩ obtained in previous experimental studies of Adams & Smith (1985; SIFDT) and Ervin & Armentrout (1987; GIB).
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Temperature dependencies of the reaction rate coefficients ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDa}}﹩, ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDb}}﹩, ﹩{k}_{{{\rm{N}}}^{+}}^{{{\rm{D}}}_{2}}﹩ obtained in the present work in comparison with ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{p}}\text{-}{{\rm{H}}}_{2}}﹩ and ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{o}}\text{-}{{\rm{H}}}_{2}}﹩ derived from the data by Zymak et al. (2013). The corresponding rate coefficients obtained from the fitted global model (model C in Table 2) are indicated by the solid curves (only the model values of ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{o}}\text{-}{{\rm{H}}}_{2}}﹩ are indicated by a dotted line to differentiate them from the nearly identical ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDa}}﹩ curve).